The parameter ranges of I-type BVFs are, \(S\) =0.26–3.1 pc, \(\Delta {V}\) =5–33 \(\rm {km\ s^{-1}}\) , \(M\) =22–4500 \(M_\odot \) , \(t_{\rm {dyn}}\) =\(5.7\!\times 10^{4}\) –\(1.2\times 10^{6}\)  yr, and \(E_{\rm {kin}}\) =\(3.4\times 10^{45}\) –\(1.8\times 10^{48}\)  erg. These are reasonably overlapped with those of protostellar outflows (e.g., [1]}; [2]}; ; [3]}; [4]}). The absence of less energetic BVFs may be a result of selection effect from different survey sensitivities. The non-I-type BVF, CO 16.134–0.553, which have a kinetic energy well greater than the range of protostellar outflows, will be discussed in §4.2. We also checked the color of the associated infrared sources (e.g., [5]}, [6]}). Most infrared sources associated with BVFs have more pronounced emission in the shorter wavelengths than in the longer wavelengths. This behavior is common for YSOs.
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